In Fig. 4a we show the Love number \(k_2\)  as a function of the compactness
\(C\) .
We expect that a very compact star for any EoS is harder to deform then
a less compact one. This is what we see in the figures.
It is interesting to observe that the same variation of \(\mathcal {B_{QCD}}\) 
and \(\xi \)  which produces visible effects in the equation of state and in the
mass-radius diagram does not lead to appreciable differences in the
\(k_2\) -\(C\)  plot. The curves shown in Fig. 4a are practically identical
to the curves
in the analogous plots shown in Refs. [1]}, [2]} and
[3]}, which were
obtained with strange quark matter equations of state. This suggests that a wide
variety of quark matter EOSs lead to the same values of \(k_2\) . We also note
that our curves are close to the one obtained with the
ultrarelativistic EOS with the speed of sound \(c^2_s =1/3\)  [3]}.
For completeness, in Fig. 4b we show the Love number \(k_2\)  as a function of
the variable \(y\) .
<FIGURE>